Molecular Bubble and Outflow in S Mon Revealed by Multiband Data Sets

• Published in: The Astrophysical journal Vol. 964; no. 1; pp. 93 - 113
• Main Authors: Liu, Dejian, Xu, Ye, Li, YingJie, Lin, Zehao, Hao, Chaojie, Yang, WenJin, Li, Jingjing, Liu, Xinrong, Dong, Yiwei, Bian, Shuaibo, Kong, Deyun
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.03.2024; IOP Publishing
• Subjects: Binary stars; Bubbles; Interstellar molecules; Kinetic energy; Massive stars; Molecular gases; Outflow; Star & galaxy formation; Star formation; Stars; Stellar wind bubbles; Stellar winds; Turbulence; Turbulent energy; Wind power; Young stellar objects
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad24e0

We identify a molecular bubble, and study the star formation and its feedback in the S Mon region, using multiple molecular lines, young stellar objects (YSOs), and infrared data. We revisit the distance to S Mon, ∼722 ± 9 pc, using Gaia Data Release 3 parallaxes of the associated Class II YSOs. The bubble may be mainly driven by a massive binary system (namely 15 Mon), the primary of which is an O7V-type star. An outflow is detected in the shell of the bubble, suggesting ongoing star formation activities in the vicinity of the bubble. The total wind energy of the massive binary star is 3 orders of magnitude higher than the sum of the observed turbulent energy in the molecular gas and the kinetic energy of the bubble, indicating that stellar winds help to maintain the turbulence in the S Mon region and drive the bubble. We conclude that the stellar winds of massive stars have an impact on their surrounding environment.